Recent observational data suggest that the expansion of the universe is accelerating. These data are confirmed by different sources, such as cosmic observations from Supernovae Ia [1]}, [2]}, Cosmic Microwave Background (CMB) radiation [3]}, [4]}, [5]}, Large Scale Structure (LSS) [6]}, weak lensing [7]}, among others. These observations are not properly explained by General Relatvity (GR). A natural question then arises: how can this acceleration be explained? To reconcile observations data and a theory that describes gravity, two main approaches are considered. That is, the observed accelerated expansion of the universe is due to some kind of extra fluid-like contribution, known as dark energy [8]}, [9]}, [10]}, or GR itself is modified [11]}. These modified theories represent a generalization of GR where some combination of curvature invariants (such as the Riemann tensor, the Weyl tensor, the Ricci tensor, among others) replaces or is added into the classical Hilbert-Einstein action, that is composed by the Ricci scalar term. For a review of modified theories of gravity, see [11]}, [13]}, [14]}, [15]}. In this paper, the \(f(R,T)\)  gravity theory is explored.
